Numerical Simulation of Active Galactic Nuclei Feedback in Galaxy NGC 5252

• Main Author: Mr. Manus Boonmalai
• Other Authors: Asst. Prof. Dr. Suwicha Wannawichian
• Format: Theses and Dissertations
• Language: English
• Published: เชียงใหม่ : บัณฑิตวิทยาลัย มหาวิทยาลัยเชียงใหม่ 2020
• Online Access: http://cmuir.cmu.ac.th/jspui/handle/6653943832/69673
• Institution: Chiang Mai University

This research aims to study the gas feedback, which can be observed the ionized gas flows out more than 10 kpc from the nucleus of Active Galactic Nuclei in NGC 5252 by use GADGET-2 program. The simulation contains gaseous disk, dark matter halo, stellar disk, and stellar bulge particles. The one of bulge particle mass is set up as the black hole mass. The simulation is used Smoothed Particle Hydrodynamics method to calculate the evolution of gaseous particles. Our simulations use only the gravitational effect from the central black hole and gas interactions to trigger the system. They do not contain factors such as the merging of the galaxy or tidal disruption. We analyze and track the distributions, internal energy, and dynamical evolutions of the gaseous disk, dark matter halo, stellar disk, and stellar bulge particles, especially its indication of the outflow and feedback process. At the beginning of the simulation, the density of each particle type undergoes the expected gravitational collapse at a small distance from the galactic center and gradually reaches its equilibrium state at around 0.6 Gyr. Our results suggest a clear indication of gas outflow in the direction perpendicular to the galactic plane. The gas can travel out more than 10 kpc in the direction perpendicular to the galactic disk after 1.6 Gyr and can travel out to 20 kpc after 3.0 Gyr. At the end of the simulations, the density of gaseous disk in the direction perpendicular to the galactic disk has increased by approximately 119 M⊙/kpc3 at distance more than 10 kpc from t = 0 to 7.0 Gyr. We see evidence in velocity in the perpendicular to disk plane direction to relate with the outflow gas of the system. The velocity of gaseous disk velocity shows a significant change from collapse at 0.01 Gyr to outflow at 0.03 Gyr. It represents the typical duty cycle of AGN. We see the feedback from the gaseous particle is more than the stellar particle. The frequency of interaction in gaseous particles is more than the stellar particles. The collision between gaseous particles leads to energy and momentum transfer. The energy of the gaseous is heated up from the interaction and kicked off from the system in the form of the outflow gas. We can see the gas feedback clearly in the perpendicular to the disk plane direction more than the disk plane direction.